By Bernard Guinot (auth.), Heinrich K. Eichhorn, Robert J. Leacock (eds.)
Read Online or Download Astrometric Techniques: Proceedings of the 109th Symposium of the International Astronomical Union Held in Gainesville, Florida, U.S.A., 9–12 January 1984 PDF
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Additional info for Astrometric Techniques: Proceedings of the 109th Symposium of the International Astronomical Union Held in Gainesville, Florida, U.S.A., 9–12 January 1984
Ashby and Allan (1979). At the epoch to pf cpprdinate time let the clocks 1,2,3 be synchronized. This means that the readings '1 '1' '1 ,respectively, in their individual proper times conform to the epoch tQ of coordinate time. The satellite 1 transmits signals periodic in its proper time ,. ConsIder a signal emitted by the sate1Hte at the moment '2 in its own time-scale, and received by the user at the moment '2 in the user's time-scale ,'. The corresponding epochs of coordinate time are t1 and t2' respectively.
Xi ~)2 I' (44) In this metric, Eq. (17) is split in the following way: dl' =! +";' 1 [Y - a('~ldg' +:: [a(el - ,a'(el] (! l(r)J~. 1 ·(g) 2 2 \ dt - c1 - 2"3 (!.. g ) - ~ 2 c r 8c dg)' +) (~dg)', 1 + r Lr:Y ~ - a. ~) (46) With the aid of Eqs. (10), (39) and (45) the relation Eq. (21) results in the final expression for the angle between two light rays (Brumberg 1981a) (y + 1) !. x £2 ) ( ) m (!. x £1 r r - -r -1 cr - r - r cr £1 x £2 . --2 (47) This formula describes the aberration effects of the first and second order together with the light deflection effect.
One may achieve the same goal, however, by substituting into Eq. (1) the expression Eq. (10) with R(t) being that function of time which defines the motion of the observer (for example, annual and diurnal motion of the Earth). 12. :
Astrometric Techniques: Proceedings of the 109th Symposium of the International Astronomical Union Held in Gainesville, Florida, U.S.A., 9–12 January 1984 by Bernard Guinot (auth.), Heinrich K. Eichhorn, Robert J. Leacock (eds.)